Aims. We describe the observing strategy, data reduction tools, and early results of a supernova (SN) search project, named SUDARE, conducted with the ESO VST telescope, which is aimed at measuring the rate of the different types of SNe in the redshift range 0.2 < z < 0.8. Methods. The search was performed in two of the best studied extragalactic fields, CDFS and COSMOS, for which a wealth of ancillary data are available in the literature or in public archives. We developed a pipeline for the data reduction and rapid identification of transients. As a result of the frequent monitoring of the two selected fields, we obtained light curve and colour information for the transients sources that were used to select and classify SNe by means of an especially developed tool. To accurately characterise the surveyed stellar population, we exploit public data and our own observations to measure the galaxy photometric redshifts and rest frame colours. Results. We obtained a final sample of 117 SNe, most of which are SN Ia (57%) with the remaining ones being core collapse events, of which 44% are type II, 22% type IIn and 34% type Ib/c. To link the transients, we built a catalogue of ~1.3 × 105 galaxies in the redshift range 0 < z ≤ 1, with a limiting magnitude KAB = 23.5 mag. We measured the SN rate per unit volume for SN Ia and core collapse SNe in different bins of redshifts. The values are consistent with other measurements from the literature. Conclusions. The dispersion of the rate measurements for SNe-Ia is comparable to the scatter of the theoretical tracks for single degenerate (SD) and double degenerate (DD) binary systems models, therefore it is not possible to disentangle among the two different progenitor scenarios. However, among the three tested models (SD and the two flavours of DD that either have a steep DDC or a wide DDW delay time distribution), the SD appears to give a better fit across the whole redshift range, whereas the DDC better matches the steep rise up to redshift ~1.2. The DDW instead appears to be less favoured. Unlike recent claims, the core collapse SN rate is fully consistent with the prediction that is based on recent estimates of star formation history and standard progenitor mass range.

Data Reduction

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THE YELLOW SUPERGIANT PROGENITOR OF THE TYPE II SUPERNOVA 2011dh IN M51

The Astrophysical Journal Letters (2011)

J. R. Maund M. Fraser M. Ergon A. Pastorello S. J. Smartt

We present the detection of the putative progenitor of the Type IIb SN 2011dh in archival pre-explosion Hubble Space Telescope images. Using post-explosion Adaptive Optics imaging with Gemini NIRI+ALTAIR, the position of the supernova (SN) in the pre-explosion images was determined to within 23 mas. The progenitor candidate is consistent with an F8 supergiant star (logL/L☉ = 4.92 ± 0.20 and Teff = 6000 ± 280 K). Through comparison with stellar evolution tracks, this corresponds to a single star at the end of core C-burning with an initial mass of MZAMS = 13 ± 3 M☉. The possibility of the progenitor source being a cluster is rejected, on the basis of: (1) the source not being spatially extended, (2) the absence of excess Hα emission, and (3) the poor fit to synthetic cluster spectral energy distributions (SEDs). It is unclear if a binary companion is contributing to the observed SED, although given the excellent correspondence of the observed photometry to a single star SED we suggest that the companion does not contribute significantly. Early photometric and spectroscopic observations show fast evolution similar to the transitional Type IIb SN 2008ax and suggest that a large amount of the progenitor's hydrogen envelope was removed before explosion. Late-time observations will reveal if the yellow supergiant or the putative companion star were responsible for this SN explosion.

10.1088/2041-8205/739/2/l37

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Citations (144)

LIGO/Virgo G274296: GRAWITA-Campo Imperatore observation

GRB Coordinates Network (2017)

A. Giunta A. Di Paola Mauro Centrone N. Napoleone P. Tedesco

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TYPE IIP SUPERNOVA 2009kf: EXPLOSION DRIVEN BY BLACK HOLE ACCRETION?

The Astrophysical Journal Letters (2010)

В. П. Утробин Н. Н. Чугай M. T. Botticella

The unusually bright type IIP supernova (SN) 2009kf is studied employing hydrodynamic modeling. We derived optimal values of the ejecta mass of 28.1 M☉, explosion energy of 2.2 × 1052 erg, and presupernova radius of 2 × 103 R☉ assuming that 56Ni mass is equal to the upper limit of 0.4 M☉. We analyzed effects of the uncertainties in the extinction and 56Ni mass and concluded that both the ejecta mass and explosion energy cannot be significantly reduced compared with the optimal values. The huge explosion energy of SN 2009kf indicates that the explosion is caused by the same mechanism which operates in energetic SNe Ibc (hypernovae), i.e., via a rapid disk accretion onto black hole. The ejecta mass combined with the black hole mass and the mass lost by stellar wind yields the progenitor mass of about 36 M☉. We propose a scenario in which massive binary evolution might result in the SN 2009kf event.

Black hole (networking)

Mass ratio

Hypernova

10.1088/2041-8205/723/1/l89

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Citations (25)

VizieR Online Data Catalog: Optical/NIR photometry of OGLE-2012-SN-006 (Pastorello+, 2015)

VizieR Online Data Catalog (2017)

A. Pastorello Ł. Wyrzykowski S. Valenti J. L. Prieto S. Kozłowski

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Psn J12211796+1130252 in NGC 4294

CBET (2013)

A. Dimai L. Tomasella P. Ochner S. Benetti A. Pastorello

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SN 2008S: an electron-capture SN from a super-AGB progenitor?

Monthly Notices of the Royal Astronomical Society (2009)

M. T. Botticella A. Pastorello S. J. Smartt W. P. S. Meikle S. Benetti

We present comprehensive photometric and spectroscopic observations of the faint transient SN 2008S discovered in NGC 6946. SN 2008S exhibited slow photometric evolution and almost no spectral variability during the first nine months, implying a high density CS medium. The light curve is similar in shape to that of SN 1998S and SN 1979C, although significantly fainter at maximum light. Our quasi-bolometric lightcurve extends to 300 days and shows a tail phase decay rate consistent with that of ^{56}Co. We propose that this is evidence for an explosion and formation of ^{56}Ni (0.0015 +/- 0.0004 M_Sun). The large MIR flux detected shortly after explosion can be explained by a light echo from pre-exisiting dust. The late NIR flux excess is plausibly due to a combination of warm newly-formed ejecta dust together with shock-heated dust in the CS environment. We reassess the progenitor object detected previously in Spitzer archive images, supplementing this discussion with a model of the MIR spectral energy distribution. This supports the idea of a dusty, optically thick shell around SN 2008S with an inner radius of nearly 90AU and outer radius of 450AU, and an inferred heating source of 3000 K and luminosity of L ~ 10^{4.6} L_Sun. The combination of our monitoring data and the evidence from the progenitor analysis leads us to support the scenario of a weak electron capture supernova explosion in a super-AGB progenitor star (of initial mass 6-8 M_sun) embedded within a thick CS gaseous envelope. We suggest that all of main properties of the electron capture SN phenomenon are observed in SN 2008S and future observations may allow a definitive answer.

Spectral energy distribution

Pair-instability supernova

Circumstellar dust

Extinction (optical mineralogy)

10.1111/j.1365-2966.2009.15082.x

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Citations (138)

SN 2009ip à la PESSTO: no evidence for core collapse yet★

Monthly Notices of the Royal Astronomical Society (2013)

M. Fraser C. Inserra A. Jerkstrand R. Kotak G. Pignata

We present ultraviolet, optical and near-infrared observations of the interacting transient SN 2009ip, covering the period from the start of the outburst in 2012 October until the end of the 2012 observing season. The transient reached a peak magnitude of MV = −17.7 mag, with a total integrated luminosity of 1.9 × 1049 erg over the period of 2012 August–December. The light curve fades rapidly, dropping by 4.5 mag from the V-band peak in 100 d. The optical and near-infrared spectra are dominated by narrow emission lines with broad electron scattering wings, signalling a dense circumstellar environment, together with multiple components of broad emission and absorption in H and He at velocities in the range 0.5–1.2 × 104 km s−1. We see no evidence for nucleosynthesized material in SN 2009ip, even in late-time pseudo-nebular spectra. We set a limit of <0.02 M⊙ on the mass of any possible synthesized 56Ni from the late-time light curve. A simple model for the narrow Balmer lines is presented and used to derive number densities for the circumstellar medium in the range ∼109–1010 cm−3. Our near-infrared data do not show any excess at longer wavelengths, and we see no other signs of dust formation. Our last data, taken in 2012 December, show that SN 2009ip has spectroscopically evolved to something quite similar to its appearance in late 2009, albeit with higher velocities. It is possible that neither of the eruptive and high-luminosity events of SN 2009ip were induced by a core collapse. We show that the peak and total integrated luminosity can be due to the efficient conversion of kinetic energy from colliding ejecta, and that around 0.05–0.1 M⊙ of material moving at 0.5–1 × 104 km s−1 could comfortably produce the observed luminosity. We discuss the possibility that these shells were ejected by the pulsational pair instability mechanism, in which case the progenitor star may still exist, and will be observed after the current outburst fades. The long-term monitoring of SN 2009ip, due to its proximity, has given the most extensive data set yet gathered of a high-luminosity interacting transient and its progenitor. It is possible that some purported Type IIn supernovae are in fact analogues of the 2012b event and that pre-explosion outbursts have gone undetected.

Balmer series

10.1093/mnras/stt813

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LIGO/Virgo S190510g: GRAWITA REM optical observations.

GRB Coordinates Network (2019)

P. D’Avanzo L. Izzo S. Yang E. Palazzi S. Campana

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Euclid. I. Overview of the Euclid mission

Y. Mellier J. A. Acevedo Barroso A. Achúcarro Jiřı́ Adámek R. Adam

10.48550/arxiv.2405.13491

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Citations (11)